1. Spectral Energy Distributions of obscured AGN E. Lusso, A. Comastri, E. Treister, D. Sanders, H. Hao, M. Elvis, C. Vignali, R. Gilli, G.Zamorani, M. Brusa, F. Civano, …

2. Outline Key Scientific Goal of AGN WG: AGN Bolometric Luminosity Function X-ray selected Type 1 AND Type 2 Bolometric luminosities and Bolometric corrections SMBH properties (Mass, Accretion Rate) vs Host Galaxies parameters (Stellar mass, SFR, morphology

3. Type 1 SED Elvis, Hao+10 Red dashed line Elvis+94 Blue lines Galaxy templates Polletta+07

4. Optical to X-ray ratio Lusso,AC+10

5. Bolometric Corrections The X-ray to optical index is a good proxy of Bolometric Luminosity i.e. Kelly+08

6. Eddington Ratios Red points from Vasudevan & Fabian 09 150 sources with BH mass

7. Type 2 About 250 X-ray selected (XMM) not-Type 1 AGN Hard X-ray spectra Most of them gas obscured Seyfert-like luminosities 43 < logLx < 44 0 < z < 1

8. Type 2 SEDs Host Galaxy dominated Infrared luminosityX-ray luminosity

9. SED Gandhi+09 IR high resolution VISIR/VLT nearby sample of X-ray bright AGN Strong correlation between AGN 2-10 keV X-ray luminosity and nuclear (non-stellar) IR emission at 12.3 micron Best estimate of the nuclear (non stellar) IR flux in AGN to date LMIR(Obs.)=LMIR(AGN)+LMIR(Host)

10. SED Decomposition

12. Type 2 host colors and morphologies ZESTNair Massive Hosts, “Green” colors

13. Summary Type 1 SED : Host Galaxy contribution Reddening Hot Dust Poor,… Elvis was “right” Type 2 SED : Host Dominated Host galaxy properties Nuclear SED ? (Elvis + reddening ?)